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arxiv: 2601.14976 · v1 · submitted 2026-01-21 · 🌌 astro-ph.GA

MSA-3D: Connecting the Chemical and Kinematic Structures of Galaxies at z sim 1

Mengting Ju , Xin Wang , Tucker Jones , Ivana Bari\v{s}i\'c , Juan M. Espejo Salcedo , Karl Glazebrook , Danail Obreschkow , Takafumi Tsukui
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Qianqiao Zhou Kevin Bundy Alaina Henry Matthew A. Malkan Themiya Nanayakkara Namrata Roy Xunda Sun
This is my paper

Pith reviewed 2026-05-16 12:18 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords metallicity gradientsgalaxy kinematicsradial mixingstar-forming galaxieshigh-redshift galaxiesturbulent mixingionized gasJWST observations
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The pith

Dynamically hotter disks show flatter metallicity gradients in galaxies at z~1.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper examines the link between ionized gas kinematics and gas-phase metallicity gradients in 21 star-forming galaxies at redshifts 0.5 to 1.7. It finds that disks with lower rotational support relative to dispersion display systematically flatter gradients. The anti-correlation strengthens when using effective radius over dispersion as a proxy for radial mixing time, suggesting mixing regulates chemical structure more directly than rotation alone. This produces uniformly shallow gradients across the sample, indicating efficient turbulent mixing shapes the chemical profiles of typical galaxies in this epoch.

Core claim

In 21 star-forming galaxies at 0.5 < z < 1.7 observed with JWST/NIRSpec, metallicity gradients are uniformly shallow and show a moderate anti-correlation with v/σ (r=-0.43) that strengthens to r=-0.59 when using Re/σ as a proxy for cumulative radial mixing timescale, indicating that turbulent mixing in kinematically settled disks directly regulates chemical stratification.

What carries the argument

Re/σ as proxy for radial mixing timescale, which carries a stronger anti-correlation with metallicity gradients than v/σ and indicates that mixing time regulates chemical stratification.

Load-bearing premise

Re/σ serves as a reliable proxy for radial mixing timescale without being driven by stellar mass covariances or measurement systematics in the sample of 21 galaxies.

What would settle it

A larger sample of similar galaxies in which the anti-correlation between Re/σ and metallicity gradient vanishes or reverses while holding stellar mass fixed.

Figures

Figures reproduced from arXiv: 2601.14976 by Alaina Henry, Danail Obreschkow, Ivana Bari\v{s}i\'c, Juan M. Espejo Salcedo, Karl Glazebrook, Kevin Bundy, Matthew A. Malkan, Mengting Ju, Namrata Roy, Qianqiao Zhou, Takafumi Tsukui, Themiya Nanayakkara, Tucker Jones, Xin Wang, Xunda Sun.

Figure 1
Figure 1. Figure 1: Two-dimensional surface brightness modeling of galaxy ID 8942 using GALFIT. The top row shows the JWST/NIRCam F444W imaging; the bottom row shows the HST/WFC3 F160W imaging. From left to right, the panels display the observed image, the best-fit S´ersic model, and the residual map after model subtraction. The fitting region is ∼ 2 ′′ × 2 ′′ box. The same color scale is used in all panels. The photometric c… view at source ↗
Figure 2
Figure 2. Figure 2: Hα velocity fields of the resolved MSA-3D galaxies at 0.5 < z < 1.7 shown at their approximate locations in the SFR-M∗ plane. The solid line indicates the star-forming main sequence from Whitaker et al. (2014) at z ∼ 1, while the dashed and dotted lines show offsets by factors of ×4 and ×10 [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Example of kinematic modeling for galaxy ID 8942. From left to right: the composite imaging cutout (used for GALFIT modeling), the observed Hα velocity field, the best-fit velocity model assuming a rotating disk, and the residual map (data minus model). The observed velocity field exhibits a rotation-dominated morphology with a spider-like pattern. The residual map confirms the quality of the fit, with a r… view at source ↗
Figure 5
Figure 5. Figure 5: Intrinsic velocity dispersion σ0 as a function of redshift. Blue filled circles represent the MSA-3D sample (this work). Galaxy 8512 is shown as a blue point with a red edge in this work, while the purple hexagon indi￾cates the result from Bariˇsi´c et al. (2025). Other samples shown for comparison are KMOS3D (diamonds; Wisnioski et al. 2015), and CO-based measurements from CO-PHIBSS (open triangles; Tacco… view at source ↗
Figure 6
Figure 6. Figure 6: Metallicity gradient (dex/kpc) as a function of the dynamical support parameter v/σ (from Hα) for our MSA-3D galaxies, shown as filled circles color-coded by stellar mass. Comparison samples are from Leethochawalit et al. (2016, open triangles), Sharda et al. (2021, small light brown), and the TNG50 simulations density histogram (grey shaded; Hemler et al. 2021) and the median trends from FIRE-2 (magenta b… view at source ↗
Figure 7
Figure 7. Figure 7: Metallicity gradient versus Re/σ for the MSA￾3D sample. Galaxies with smaller Re/σ show systematically flatter metallicity gradients, whereas systems with larger Re/σ tend to exhibit more negative gradients. The Pear￾son correlation coefficient is r = -0.59 (p = 0.005). are successfully fitted, yielding their rotation velocities (vrot) and intrinsic velocity dispersions (σ0); requiring a reliable measureme… view at source ↗
read the original abstract

We investigate the connection between ionized gas kinematics and gas-phase metallicity gradients in 21 star-forming galaxies at $0.5 < z < 1.7$ from the MSA-3D survey, using spatially resolved JWST/NIRSpec slit-stepping observations. Galaxy kinematics are characterized by the ratio of rotational velocity to intrinsic velocity dispersion, $v/\sigma$, measured at $1.5\,R_e$, where $R_e$ is the effective radius. We find that dynamically hotter disks exhibit systematically flatter metallicity gradients, with a moderate anti-correlation between metallicity gradient and $v/\sigma$ (Pearson $r=-0.43$, $p=0.05$) and a linear fit yields a slope of $\sim 0.005$ dex per dex in $v/\sigma$, weaker than the dependence on stellar mass. A significantly stronger anti-correlation is observed with $R_e/\sigma$, interpreted as a proxy for the radial mixing timescale ($r=-0.59$, $p=0.005$), indicating that cumulative radial mixing more directly regulates chemical stratification. The metallicity gradients in our sample are uniformly shallow, indicating that efficient turbulent mixing in kinematically settled disks regulates the chemical structure of typical star-forming galaxies at $z\sim1$.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 2 minor

Summary. The manuscript reports observations of 21 star-forming galaxies at 0.5 < z < 1.7 using JWST/NIRSpec slit-stepping data. It measures ionized-gas kinematics via v/σ at 1.5 Re and gas-phase metallicity gradients, finding a moderate anti-correlation between the gradient and v/σ (Pearson r = -0.43, p = 0.05) with a linear-fit slope of ~0.005 dex per dex, and a stronger anti-correlation with Re/σ (r = -0.59, p = 0.005). The gradients are uniformly shallow; the authors interpret Re/σ as a proxy for cumulative radial-mixing timescale that more directly regulates chemical stratification than v/σ alone.

Significance. If the correlations survive controls for stellar mass and selection, the result supplies direct observational evidence linking disk kinematics to chemical evolution at the peak of cosmic star formation. The JWST spatially resolved spectroscopy and the uniform shallowness of the gradients are notable strengths that could constrain turbulent-mixing models.

major comments (2)
  1. [Results / correlation analysis] The central claim that 'cumulative radial mixing more directly regulates chemical stratification' rests on Re/σ showing a stronger anti-correlation than v/σ. No partial-correlation coefficients or multivariate regression controlling for stellar mass (explicitly noted in the text as driving steeper trends) are presented; without this control the causal interpretation is not yet secured.
  2. [Methods and statistical analysis] N = 21 is modest; the reported p = 0.005 for the Re/σ correlation requires explicit robustness checks (bootstrap or jackknife uncertainties on r, or leave-one-out tests) to demonstrate that the result is not driven by a few points or by sample selection.
minor comments (2)
  1. [Abstract and Results] The linear-fit slope is quoted as '~0.005 dex per dex' without formal uncertainties or the exact fitting method (ordinary least squares, errors-in-variables, etc.); these details should be supplied.
  2. [Figures] Figures showing gradient versus v/σ and Re/σ should include individual-point error bars, the fitted line with confidence band, and the Pearson r and p values directly on the panels for clarity.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive comments, which help strengthen the statistical robustness and causal interpretation of our results. We address each major point below and will revise the manuscript accordingly.

read point-by-point responses

  1. Referee: The central claim that 'cumulative radial mixing more directly regulates chemical stratification' rests on Re/σ showing a stronger anti-correlation than v/σ. No partial-correlation coefficients or multivariate regression controlling for stellar mass (explicitly noted in the text as driving steeper trends) are presented; without this control the causal interpretation is not yet secured.

    Authors: We agree that explicit controls for stellar mass are needed to secure the interpretation that Re/σ more directly regulates chemical stratification. In the revised manuscript we will add partial-correlation coefficients between metallicity gradient and Re/σ (controlling for stellar mass) and a multivariate linear regression that includes both Re/σ and stellar mass as predictors. These analyses will quantify the independent contribution of Re/σ and will be reported in the results section with updated figures and tables. revision: yes

  2. Referee: N = 21 is modest; the reported p = 0.005 for the Re/σ correlation requires explicit robustness checks (bootstrap or jackknife uncertainties on r, or leave-one-out tests) to demonstrate that the result is not driven by a few points or by sample selection.

    Authors: We acknowledge the modest sample size and the importance of demonstrating robustness. In the revision we will include bootstrap resampling (with 10,000 iterations) and jackknife estimates of the Pearson r and its uncertainty for the Re/σ correlation, together with leave-one-out tests that show the correlation coefficient and p-value remain stable when any single galaxy is removed. These checks will be added to the methods and results sections. revision: yes

Circularity Check

0 steps flagged

No significant circularity: purely observational correlations from new data

full rationale

The paper reports direct measurements of v/σ and Re/σ from JWST/NIRSpec observations of 21 galaxies, then computes Pearson correlations and a linear fit slope against independently measured metallicity gradients. No equations, predictions, or parameters are defined in terms of the target result; the reported anti-correlations (r = -0.43 and -0.59) are statistical outputs from the data, not inputs renamed as outputs. No self-citations, uniqueness theorems, or ansatzes are invoked to justify the central claims. The analysis is self-contained against external benchmarks and does not reduce any derivation to its own fitted values by construction.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

Central claim rests on standard assumptions that v/σ at 1.5 Re captures disk dynamical state and that Re/σ proxies mixing timescale; one fitted slope parameter is introduced for the linear relation.

free parameters (1)
  • linear fit slope ~0.005 dex per dex
    Slope of the reported relation between metallicity gradient and v/σ is obtained by fitting the observed data points.
axioms (2)
  • domain assumption v/σ measured at 1.5 Re accurately represents the dynamical state of the disk
    Invoked when characterizing kinematics for the correlation analysis.
  • domain assumption Re/σ serves as a proxy for radial mixing timescale
    Used to interpret the stronger correlation as evidence for mixing regulation.

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Works this paper leans on

64 extracted references · 64 canonical work pages · 1 internal anchor

  1. [1]

    L., Birkin, J

    Amvrosiadis, A., Wardlow, J. L., Birkin, J. E., et al. 2025, MNRAS, 536, 3757, doi: 10.1093/mnras/stae2760 Bariˇ si´ c, I., Jones, T., Mortensen, K., et al. 2025, ApJ, 983, 139, doi: 10.3847/1538-4357/ada617

    work page doi:10.1093/mnras/stae2760 2025

  2. [2]

    A., Wetzel, A., Loebman, S

    Bellardini, M. A., Wetzel, A., Loebman, S. R., & Bailin, J. 2022, MNRAS, 514, 4270, doi: 10.1093/mnras/stac1637

    work page doi:10.1093/mnras/stac1637 2022

  3. [3]

    A., Wetzel, A., Loebman, S

    Bellardini, M. A., Wetzel, A., Loebman, S. R., et al. 2021, MNRAS, 505, 4586, doi: 10.1093/mnras/stab1606

    work page doi:10.1093/mnras/stab1606 2021

  4. [4]

    B., van Dokkum, P

    Brammer, G. B., van Dokkum, P. G., Franx, M., et al. 2012, ApJS, 200, 13, doi: 10.1088/0067-0049/200/2/13

    work page doi:10.1088/0067-0049/200/2/13 2012

  5. [5]

    M., Genzel, R., et al

    Burkert, A., F¨ orster Schreiber, N. M., Genzel, R., et al. 2016, ApJ, 826, 214, doi: 10.3847/0004-637X/826/2/214

    work page doi:10.3847/0004-637x/826/2/214 2016

  6. [6]

    2010, Nature, 467, 811, doi: 10.1038/nature09451

    Cresci, G., Mannucci, F., Maiolino, R., et al. 2010, Nature, 467, 811, doi: 10.1038/nature09451

    work page doi:10.1038/nature09451 2010

  7. [7]

    L., Tacchella, S., Übler, H., et al

    Danhaive, A. L., Tacchella, S., ¨Ubler, H., et al. 2025, MNRAS, 543, 3249, doi: 10.1093/mnras/staf1540

    work page doi:10.1093/mnras/staf1540 2025

  8. [8]

    I., Tacconi, L

    Davies, R. I., Tacconi, L. J., & Genzel, R. 2004, ApJ, 602, 148, doi: 10.1086/380995 de Graaff, A., Rix, H.-W., Carniani, S., et al. 2024, A&A, 684, A87, doi: 10.1051/0004-6361/202347755

    work page doi:10.1086/380995 2004

  9. [9]

    R., Audibert, A., et al

    Esparza-Arredondo, D., Ramos Almeida, C., Audibert, A., et al. 2025, A&A, 693, A174, doi: 10.1051/0004-6361/202452488 Faucher-Gigu` ere, C.-A., Kereˇ s, D., & Ma, C.-P. 2011, MNRAS, 417, 2982, doi: 10.1111/j.1365-2966.2011.19457.x

    work page doi:10.1051/0004-6361/202452488 2025

  10. [10]

    2014 , month = feb, journal =

    Forbes, J. C., Krumholz, M. R., Burkert, A., & Dekel, A. 2014, MNRAS, 438, 1552, doi: 10.1093/mnras/stt2294 F¨ orster Schreiber, N. M., Renzini, A., Mancini, C., et al. 2018, ApJS, 238, 21, doi: 10.3847/1538-4365/aadd49

    work page doi:10.1093/mnras/stt2294 2014

  11. [11]

    Furlanetto, S. R. 2021, MNRAS, 500, 3394, doi: 10.1093/mnras/staa3451

    work page doi:10.1093/mnras/staa3451 2021

  12. [12]

    M., Torrey, P., Bhagwat, A., et al

    Garcia, A. M., Torrey, P., Bhagwat, A., et al. 2025, arXiv e-prints, arXiv:2503.03804, doi: 10.48550/arXiv.2503.03804

    work page doi:10.48550/arxiv.2503.03804 2025

  13. [13]

    K., Pilkington, K., Brook, C

    Gibson, B. K., Pilkington, K., Brook, C. B., Stinson, G. S., & Bailin, J. 2013, A&A, 554, A47, doi: 10.1051/0004-6361/201321239

    work page doi:10.1051/0004-6361/201321239 2013

  14. [14]

    M., Tiley, A

    Gillman, S., Swinbank, A. M., Tiley, A. L., et al. 2019, MNRAS, 486, 175, doi: 10.1093/mnras/stz765

    work page doi:10.1093/mnras/stz765 2019

  15. [15]

    L., Swinbank, A

    Gillman, S., Tiley, A. L., Swinbank, A. M., et al. 2021, MNRAS, 500, 4229, doi: 10.1093/mnras/staa3400

    work page doi:10.1093/mnras/staa3400 2021

  16. [16]

    A., Fontana, A., et al

    Girard, M., Mason, C. A., Fontana, A., et al. 2020, MNRAS, 497, 173, doi: 10.1093/mnras/staa1907

    work page doi:10.1093/mnras/staa1907 2020

  17. [17]

    S., Torrey, P., Qi, J., et al

    Hemler, Z. S., Torrey, P., Qi, J., et al. 2021, MNRAS, 506, 3024, doi: 10.1093/mnras/stab1803

    work page doi:10.1093/mnras/stab1803 2021

  18. [18]

    2010, ApJL, 725, L176, doi: 10.1088/2041-8205/725/2/L176

    Jones, T., Ellis, R., Jullo, E., & Richard, J. 2010, ApJL, 725, L176, doi: 10.1088/2041-8205/725/2/L176

    work page doi:10.1088/2041-8205/725/2/l176 2010

  19. [19]

    S., Richard J., Jullo E., 2013, @doi [ ] 10.1088/0004-637X/765/1/48 , https://ui.adsabs.harvard.edu/abs/2013ApJ...765...48J 765, 48

    Jones, T., Ellis, R. S., Richard, J., & Jullo, E. 2013, ApJ, 765, 48, doi: 10.1088/0004-637X/765/1/48

    work page doi:10.1088/0004-637x/765/1/48 2013

  20. [20]

    2022, ApJ, 938, 96, doi: 10.3847/1538-4357/ac9056

    Ju, M., Yin, J., Liu, R., et al. 2022, ApJ, 938, 96, doi: 10.3847/1538-4357/ac9056

    work page doi:10.3847/1538-4357/ac9056 2022

  21. [21]

    2025, ApJL, 978, L39, doi: 10.3847/2041-8213/ada150

    Ju, M., Wang, X., Jones, T., et al. 2025, ApJL, 978, L39, doi: 10.3847/2041-8213/ada150

    work page doi:10.3847/2041-8213/ada150 2025

  22. [22]

    A., Weiner, B

    Kassin, S. A., Weiner, B. J., Faber, S. M., et al. 2007, ApJL, 660, L35, doi: 10.1086/517932 —. 2012, ApJ, 758, 106, doi: 10.1088/0004-637X/758/2/106

    work page doi:10.1086/517932 2007

  23. [23]

    M., Faber, S

    Koekemoer, A. M., Faber, S. M., Ferguson, H. C., et al. 2011, ApJS, 197, 36, doi: 10.1088/0067-0049/197/2/36

    work page doi:10.1088/0067-0049/197/2/36 2011

  24. [24]

    Lange, J. U. 2023, Monthly Notices of the Royal Astronomical Society, 525, 3181, doi: 10.1093/mnras/stad2441

    work page doi:10.1093/mnras/stad2441 2023

  25. [25]

    L., F¨ orster Schreiber, N

    Lee, L. L., F¨ orster Schreiber, N. M., Price, S. H., et al. 2025, ApJ, 978, 14, doi: 10.3847/1538-4357/ad90b5 MSA-3D: gas kinematics and metallicity gradients inz∼1galaxies13 Figure A1.A comprehensive spatially-resolved view of our galaxy sample with gas kinematic information. For galaxies that have converged kinematic fits, the top row shows (from left ...

    work page doi:10.3847/1538-4357/ad90b5 2025

  26. [26]

    A., Ellis, R

    Leethochawalit, N., Jones, T. A., Ellis, R. S., et al. 2016, ApJ, 820, 84, doi: 10.3847/0004-637X/820/2/84

    work page doi:10.3847/0004-637x/820/2/84 2016

  27. [27]

    , keywords =

    Li, Z., Cai, Z., Wang, X., et al. 2025, ApJS, 280, 62, doi: 10.3847/1538-4365/adfa70

    work page doi:10.3847/1538-4365/adfa70 2025

  28. [28]

    F., Feldmann, R., et al

    Ma, X., Hopkins, P. F., Feldmann, R., et al. 2017, MNRAS, 466, 4780, doi: 10.1093/mnras/stx034

    work page doi:10.1093/mnras/stx034 2017

  29. [29]

    doi:10.1007/s00159-018-0112-2

    Maiolino, R., & Mannucci, F. 2019, A&A Rv, 27, 3, doi: 10.1007/s00159-018-0112-2

    work page doi:10.1007/s00159-018-0112-2 2019

  30. [30]

    R., Mesa-Delgado A., L \'o pez-Mart \'i n L., Esteban C., 2011, @doi [MNRAS] 10.1111/j.1365-2966.2010.17847.x , 411, 2076

    Gnerucci, A. 2010, MNRAS, 408, 2115, doi: 10.1111/j.1365-2966.2010.17291.x

    work page doi:10.1111/j.1365-2966.2010.17291.x 2010

  31. [31]

    H., Bundy, K., Sullivan, M., Ellis, R

    Miller, S. H., Bundy, K., Sullivan, M., Ellis, R. S., & Treu, T. 2011, ApJ, 741, 115, doi: 10.1088/0004-637X/741/2/115

    work page doi:10.1088/0004-637x/741/2/115 2011

  32. [32]

    H., Ellis, R

    Miller, S. H., Ellis, R. S., Sullivan, M., et al. 2012, ApJ, 753, 74, doi: 10.1088/0004-637X/753/1/74 16Ju et al. Figure A1.continued MSA-3D: gas kinematics and metallicity gradients inz∼1galaxies17 Figure A1.continued 18Ju et al. Figure A1.continued MSA-3D: gas kinematics and metallicity gradients inz∼1galaxies19 Figure A1.continued 20Ju et al. Figure A1...

    work page doi:10.1088/0004-637x/753/1/74 2012

  33. [33]

    G., Brammer, G

    Momcheva, I. G., Brammer, G. B., van Dokkum, P. G., et al. 2016, ApJS, 225, 27, doi: 10.3847/0067-0049/225/2/27

    work page doi:10.3847/0067-0049/225/2/27 2016

  34. [34]

    C., & Shetty, R

    Ostriker, E. C., & Shetty, R. 2011, ApJ, 731, 41, doi: 10.1088/0004-637X/731/1/41

    work page doi:10.1088/0004-637x/731/1/41 2011

  35. [35]

    Peng and Luis C

    Peng, C. Y., Ho, L. C., Impey, C. D., & Rix, H.-W. 2002, AJ, 124, 266, doi: 10.1086/340952 —. 2010, AJ, 139, 2097, doi: 10.1088/0004-6256/139/6/2097

    work page internal anchor Pith review doi:10.1086/340952 2002

  36. [36]

    Pettini, M., & Pagel, B. E. J. 2004, MNRAS, 348, L59, doi: 10.1111/j.1365-2966.2004.07591.x

    work page doi:10.1111/j.1365-2966.2004.07591.x 2004

  37. [37]

    2012, A&A, 539, A93, doi: 10.1051/0004-6361/201117718

    Queyrel, J., Contini, T., Kissler-Patig, M., et al. 2012, A&A, 539, A93, doi: 10.1051/0004-6361/201117718

    work page doi:10.1051/0004-6361/201117718 2012

  38. [38]

    2025, A&A, 698, A267, doi: 10.1051/0004-6361/202452658

    Ratcliffe, B., Khoperskov, S., Minchev, I., et al. 2025, A&A, 698, A267, doi: 10.1051/0004-6361/202452658

    work page doi:10.1051/0004-6361/202452658 2025

  39. [39]

    2025, arXiv e-prints, arXiv:2510.11326, doi: 10.48550/arXiv.2510.11326 MSA-3D: gas kinematics and metallicity gradients inz∼1galaxies27 Figure A1.continued 28Ju et al

    Roy, N., Henry, A., Jones, T., et al. 2025, arXiv e-prints, arXiv:2510.11326, doi: 10.48550/arXiv.2510.11326 MSA-3D: gas kinematics and metallicity gradients inz∼1galaxies27 Figure A1.continued 28Ju et al. Figure A1.continued MSA-3D: gas kinematics and metallicity gradients inz∼1galaxies29 Figure A1.continued

    work page doi:10.48550/arxiv.2510.11326 2025

  40. [40]

    R., & Federrath, C

    Sharda, P., Wisnioski, E., Krumholz, M. R., & Federrath, C. 2021, MNRAS, 506, 1295, doi: 10.1093/mnras/stab1836

    work page doi:10.1093/mnras/stab1836 2021

  41. [41]

    C., Papovich, C., Momcheva, I., et al

    Simons, R. C., Papovich, C., Momcheva, I., et al. 2021, ApJ, 923, 203, doi: 10.3847/1538-4357/ac28f4

    work page doi:10.3847/1538-4357/ac28f4 2021

  42. [42]

    E., Whitaker, K

    Skelton, R. E., Whitaker, K. E., Momcheva, I. G., et al. 2014, ApJS, 214, 24, doi: 10.1088/0067-0049/214/2/24

    work page doi:10.1088/0067-0049/214/2/24 2014

  43. [43]

    2025, ApJ, 986, 179, doi: 10.3847/1538-4357/addab5

    Sun, X., Wang, X., Ma, X., et al. 2025, ApJ, 986, 179, doi: 10.3847/1538-4357/addab5

    work page doi:10.3847/1538-4357/addab5 2025

  44. [44]

    M., Papadopoulos, P

    Swinbank, A. M., Papadopoulos, P. P., Cox, P., et al. 2011, ApJ, 742, 11, doi: 10.1088/0004-637X/742/1/11

    work page doi:10.1088/0004-637x/742/1/11 2011

  45. [45]

    J., Neri, R., Genzel, R., et al

    Tacconi, L. J., Neri, R., Genzel, R., et al. 2013, ApJ, 768, 74, doi: 10.1088/0004-637X/768/1/74

    work page doi:10.1088/0004-637x/768/1/74 2013

  46. [46]

    K., Eichler, M., Panov, I

    Thielemann, F. K., Eichler, M., Panov, I. V., & Wehmeyer, B. 2017, Annual Review of Nuclear and Particle Science, 67, 253, doi: 10.1146/annurev-nucl-101916-123246

    work page doi:10.1146/annurev-nucl-101916-123246 2017

  47. [47]

    L., Gillman, S., Cortese, L., et al

    Tiley, A. L., Gillman, S., Cortese, L., et al. 2021, MNRAS, 506, 323, doi: 10.1093/mnras/stab1692

    work page doi:10.1093/mnras/stab1692 2021

  48. [48]

    B., Rosas-Guevara, Y., Sillero, E., et al

    Tissera, P. B., Rosas-Guevara, Y., Sillero, E., et al. 2022, MNRAS, 511, 1667, doi: 10.1093/mnras/stab3644

    work page doi:10.1093/mnras/stab3644 2022

  49. [49]

    The Origin of the Mass--Metallicity Relation: Insights from 53,000 Star-Forming Galaxies in the SDSS

    Tremonti, C. A., Heckman, T. M., Kauffmann, G., et al. 2004, ApJ, 613, 898, doi: 10.1086/423264

    work page Pith review doi:10.1086/423264 2004

  50. [50]

    2025, MNRAS, 540, 3493, doi: 10.1093/mnras/staf604

    Tsukui, T., Wisnioski, E., Bland-Hawthorn, J., & Freeman, K. 2025, MNRAS, 540, 3493, doi: 10.1093/mnras/staf604

    work page doi:10.1093/mnras/staf604 2025

  51. [51]

    B., & Fisher, J

    Tully, R. B., & Fisher, J. R. 1977, A&A, 54, 661 ¨Ubler, H., Genzel, R., Wisnioski, E., et al. 2019, ApJ, 880, 48, doi: 10.3847/1538-4357/ab27cc van den Bosch, F. C. 2002, MNRAS, 331, 98, doi: 10.1046/j.1365-8711.2002.05171.x

    work page doi:10.3847/1538-4357/ab27cc 1977

  52. [52]

    2024, A&A, 691, A19, doi: 10.1051/0004-6361/202449855

    Venturi, G., Carniani, S., Parlanti, E., et al. 2024, A&A, 691, A19, doi: 10.1051/0004-6361/202449855

    work page doi:10.1051/0004-6361/202449855 2024

  53. [53]

    2024a, ApJL, 973, L29, doi: 10.3847/2041-8213/ad772d

    Wang, B., Peng, Y., Cappellari, M., Gao, H., & Mo, H. 2024a, ApJL, 973, L29, doi: 10.3847/2041-8213/ad772d

    work page doi:10.3847/2041-8213/ad772d 2041

  54. [54]

    2024b, ApJ, 970, 34, doi: 10.3847/1538-4357/ad5952

    Wang, E., Lian, J., Peng, Y., & Wang, X. 2024b, ApJ, 970, 34, doi: 10.3847/1538-4357/ad5952

    work page doi:10.3847/1538-4357/ad5952

  55. [55]

    Wang, E., & Lilly, S. J. 2023, ApJ, 955, 55, doi: 10.3847/1538-4357/acecfd

    work page doi:10.3847/1538-4357/acecfd 2023

  56. [56]

    A., Treu, T., et al

    Wang, X., Jones, T. A., Treu, T., et al. 2017, ApJ, 837, 89, doi: 10.3847/1538-4357/aa603c —. 2019, ApJ, 882, 94, doi: 10.3847/1538-4357/ab3861 —. 2020, ApJ, 900, 183, doi: 10.3847/1538-4357/abacce

    work page doi:10.3847/1538-4357/aa603c 2017

  57. [57]

    2022, ApJL, 938, L16, doi: 10.3847/2041-8213/ac959e

    Wang, X., Jones, T., Vulcani, B., et al. 2022, ApJL, 938, L16, doi: 10.3847/2041-8213/ac959e

    work page doi:10.3847/2041-8213/ac959e 2022

  58. [58]

    E., Franx, M., Leja, J., et al

    Whitaker, K. E., Franx, M., Leja, J., et al. 2014, ApJ, 795, 104, doi: 10.1088/0004-637X/795/2/104

    work page doi:10.1088/0004-637x/795/2/104 2014

  59. [59]

    T., Leaman, R., et al

    Wisnioski, E., Mendel, J. T., Leaman, R., et al. 2025, MNRAS, 544, 2777, doi: 10.1093/mnras/staf1606 30Ju et al

    work page doi:10.1093/mnras/staf1606 2025

  60. [60]

    M., & Koo, D

    Wisnioski, E., F¨ orster Schreiber, N. M., Wuyts, S., et al. 2015, ApJ, 799, 209, doi: 10.1088/0004-637X/799/2/209

    work page doi:10.1088/0004-637x/799/2/209 2015

  61. [61]

    M., Wisnioski, E., et al

    Wuyts, S., F¨ orster Schreiber, N. M., Wisnioski, E., et al. 2016, ApJ, 831, 149, doi: 10.3847/0004-637X/831/2/149

    work page doi:10.3847/0004-637x/831/2/149 2016

  62. [62]

    2012, ApJ, 758, 48, doi: 10.1088/0004-637X/758/1/48

    Yang, C.-C., & Krumholz, M. 2012, ApJ, 758, 48, doi: 10.1088/0004-637X/758/1/48

    work page doi:10.1088/0004-637x/758/1/48 2012

  63. [63]

    2024, MNRAS, 528, 5295, doi: 10.1093/mnras/stae335

    Yang, M., Zhu, L., Lei, Y., et al. 2024, MNRAS, 528, 5295, doi: 10.1093/mnras/stae335

    work page doi:10.1093/mnras/stae335 2024

  64. [64]

    T., Kewley, L

    Yuan, T. T., Kewley, L. J., Swinbank, A. M., Richard, J., & Livermore, R. C. 2011, ApJL, 732, L14, doi: 10.1088/2041-8205/732/1/L14

    work page doi:10.1088/2041-8205/732/1/l14 2011